The 2dF QSO Redshift Survey - XIV. Structure and evolution from the two-point correlation function

By Scott M. Croom, B. Boyle, T. Shanks, R. Smith, L. Miller, P. Outram, N. Loaring, F. Hoyle, J. D. A. Aao, Atnf and 6 more. 2004

341 citations recorded by the source corpus.

In this paper we present a clustering analysis of quasi-stellar objects (QSOs) using over 20 000 objects from the final catalogue of the 2dF QSO Redshift Survey (2QZ), measuring the redshift-space two-point correlation function, ξ(s). When averaged over the redshift range 0.3 < z < 2.2 we find that ξ(s) is flat on small scales, steepening on scales above ∼25 h -1 Mpc. In a WMAP/2dF cosmology (Ω m = 0.27, Ω A = 0.73) we find a best-fitting power law with so = 5.48 +0.42 -0.48 h -1 Mpc and γ = 1.20 ± 0.10 on scales s = 1 to 25 h -1 Mpc. We demonstrate that non-linear redshift-space distortions have a significant effect on the QSO ξ(s) at scales less than ∼10 h -1 Mpc. A cold dark matter model assuming WMAP/2dF cosmological parameters is a good description of the QSO ξ(s) after accounting for non-linear clustering and redshift-space distortions, and allowing for a linear bias at the mean redshift of b Q (z = 1.35) = 2.02 ± 0.07. We subdivide the 2QZ into 10 redshift intervals with effective redshifts from z = 0.53 to 2.48. We find a significant increase in clustering amplitude at high redshift in the WMAP/2dF cosmology. The QSO clustering amplitude increases with redshift such that the integrated correlation function, ξ(s), within 20 h -1 Mpc is ξ(20, z = 0.53) = 0.26 ± 0.08 and ξ(20, z = 2.48) = 0.70 ± 0.17. We derive the QSO bias and find it to be a strong function of redshift with b Q (z = 0.53) = 1.13 ± 0.18 and b Q (z = 2.48) = 4.24 ± 0.53. We use these bias values to derive the mean dark matter halo (DMH) mass occupied by the QSOs. At all redshifts 2QZ QSOs inhabit approximately the same mass DMHs with M DH = (3.0 ± 1.6) × 10 12 h -1 M ○. , which is close to the characteristic mass in the Press-Schechter mass function, M*, at z = 0. These results imply that LQ QSOs at z ∼ 0 should be largely unbiased. If the relation between black hole (BH) mass and M DH or host velocity dispersion does not evolve, then we find that the accretion efficiency (L /L Edd ) for LQ QSOs is approximately constant with redshift. Thus the fading of the QSO population from z ∼ 2 to ∼0 appears to be due to less massive BHs being active at low redshift. We apply different methods to estimate, t Q , the active lifetime of QSOs and constrain t Q to be in the range 4 x 10 6 -6 x 10 8 yr at z ∼2. We test for any luminosity dependence of QSO clustering by measuring ξ(s) as a function of apparent magnitude (equivalent to luminosity relative to L* Q ). However, we find no significant evidence of luminosity-dependent clustering from this data set.

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Citations in the corpus

• CLUSTERING OF LOW-REDSHIFT (z ⩽ 2.2) QUASARS FROM THE SLOAN DIGITAL SKY SURVEY (2008, methodology): “The (green) filled squares are from the 2QZ (Croom et al. 2005), while the (red) filled star is from a measurement of AGN clustering at z < 0.2 by Wake et al. (2004).”
• Clustering of High-Redshift (z ≥ 2.9) Quasars from the Sloan Digital Sky Survey (2007, methodology): “Studies of the clustering properties of quasars date back to Osmer (1981); in general, quasars have a clustering strength similar to that of luminous galaxies atthe same redshift (Shaver 1984; Croom & Shanks 1996; Porciani, Magliocchetti & Norberg 2004, hereafter PMN04; Croom et al. 2005).”
• THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: QUASAR TARGET SELECTION FOR DATA RELEASE NINE (2011, methodology): “The SDSS-III BOSS: Quasar Target Selection for DR9 11 are not inadvertently rejecting any real z > 2.2 quasars, since the vast majority of these objects were visually inspected and identified in the SDSS, 2QZ and MMT surveys (Schneider et al. 2010; Croom et al. 2005).”
• The Sydney-AAO Multi-object Integral field spectrograph (2011, background): “The most luminous AGN (i.e. bright quasars) require >∼10 9 solar masses of gas deposited in their central regions on timescales of ∼107–108 years (e.g. Croom et al. 2005), requiring major galaxy-wide perturbations (Hopkins & Hernquist 2009), and no doubt triggering substantial star formation.”
• QUASAR CLUSTERING FROM SDSS DR5: DEPENDENCES ON PHYSICAL PROPERTIES (2008, methodology): “…of the 2QZ (Croom et al. 2004) and the 2SLAQ (Croom et al. 2008) spectroscopic samples studied by several authors (e.g., Porciani et al. 2004; Croom et al. 2005; da Ângela et al. 2005; da Ângela et al. 2008), because SDSS does not reach as far down the quasar luminosity function as the other…”
• A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, background): “It is well established empirically that quasar clustering traces a characteristic host halo mass (Porciani et al. 2004; Wake et al. 2004; Croom et al. 2005; Porciani & Norberg 2006; Myers et al. 2007a; da Angela et al. 2007; Coil et al. 2007; Shen et al. 2007; Hopkins et al. 2007d), and…”
• THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE (2012, methodology): “Using the same arguments as in White et al. (2012), and the conversions of Croom et al. (2005) and Shen et al. (2009), we place the median BOSS quasar with a bolometric luminosity of Lbol = 2−4×10 46 erg s−1, in dark matter haloes of characteristic mass of ∼ 2 × 1012 h−1M⊙ at z ≈ 2.5.”
• A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, background): “Our predicted bias agrees well with early observational evidence from Croom et al. (2005), who also find no evidence for a dependence of the correlation on quasar luminosity at a given redshift, exactly as we predict.”
• THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: OVERVIEW AND EARLY DATA (2015, unknown): “We make BAO projections assuming a flat redshift distribution and the bias relationship b(z) = 0.53 + 0.29(1 + z)2 determined by Croom et al. (2005) and consistent with SDSS measurements (Myers et al. 2007, 2006).”
• Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources (2007, methodology): “In view of the tight connection between spheroidal galaxies and active galactic nuclei at their centers entailed by the model of Granato et al. (2004), we assume the correlation length, r0, to be constant in comoving coordinates, as suggested by quasar data (Porciani et al. 2004; Croom et al. 2005).”
• Dusty Star Forming Galaxies at High Redshift (2014, background): “The inferred halo masses for luminous SMGs and DOGs are not terribly dissimilar from constraints on optically-selected quasars (Croom et al., 2005; White et al., 2012).”
• A Measurement of the Quadrupole Power Spectrum in the Clustering of the 2dF QSO Survey (2005, methodology): “They have given the best fit formula (Croom et al.2005). b(z) = 0.53+ 0.289(1+ z)2.”
• Cosmic Homogeneity Demonstrated with Luminous Red Galaxies (2004, background): “In what follows, a cosmological world model with M ¼ 0:3, ¼ 0:7 is adopted, and the Hubble constant is parameterized H0 ¼ 100 h km s 1 Mpc 1, for the purposes of calculating distances (e.g., Hogg 1999).”
• The Completed SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations with Lyα Forests (2020, methodology): “Following the analysis of du Mas des Bourboux et al. (2019) based on a compilation of quasar bias measurements (Croom et al. 2005; Shen et al. 2013; Laurent et al. 2016, 2017), we set º =b b z 3.77q q eff( ) with a redshift dependence given by = + b z z 3.60 1 3.334 .”
• The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, methodology): “The 2dF and SDSS QSO redshift surveys have been used to study the dark matter haloes of powerful AGN to even higher redshifts (Porciani et al. 2004, Croom et al. 2005, Ross et al. 2009).”
• Clustering Analyses of 300,000 Photometrically Classified Quasars. I. Luminosity and Redshift Evolution in Quasar Bias (2006, background): “…(e.g., Hopkins et al. 2006), this picture is consistent with emerging evidence that at z ∼< 2.5 quasar bias evolves with redshift but that quasars inhabit dark matter halos of similar average mass at every redshift (Porciani, Magliocchetti & Norberg 2004; Croom et al. 2005; Myers et al. 2006).”
• The DEEP3 Galaxy Redshift Survey: the impact of environment on the size evolution of massive early-type galaxies at intermediate redshift (2011, background): “In addition, Croom et al. (2005) find that the average dark matter halo mass for quasars at intermediate redshift is roughly consistent with (within a factor of a few) the minimum halo mass inferred for groups at z ∼ 1 (Coil et al. 2006, see also Hopkins et al. 2007).”
• Neutral hydrogen in galaxy haloes at the peak of the cosmic star formation history (2014, background): “These halos bracket the characteristic mass MQSO = 3 × 1012 M of quasar-hosting halos at z ∼ 2 (e.g., Croom et al. 2005; White et al. 2012).”